VizieR Online Data Catalog: SNe Ia light curves for the LSQ-CSP sample (Walker+, 2015)
Abstract
All of the supernovae described in this paper were discovered in the La Silla/QUEST Southern Hemisphere Variability Survey and were classified spectroscopically as SNe Ia by a variety of larger telescopes. The spectra are available on the WISEREP database (Yaron & Gal-Yam 2012PASP..124..668Y). The supernovae published here were followed photometrically in multiple filter bands using the Swope telescope at the Las Campanas Observatory to construct the light curves covering the period around maximum light.
The La Silla/QUEST survey started the Low Redshift Supernova Search in 2011 December (Baltay et al. 2013PASP..125..683B). The survey uses the 1m ESO Schmidt telescope at the La Silla Observatory in Chile. The spectroscopy used to classify the supernova candidates was carried out using five different telescopes. The spectra taken for this sample of supernovae that had peak brightness before 2013 May are: ------------------------------------------------------------------ Source Telescope Spectrometer No. of SNe ------------------------------------------------------------------ PESSTO 3.5m NTT EFOSC-II 12 CSP II 2.5m du Pont WFCCD 10 SNfactory 2.2m UHT SNIFS 8 LCOGT 2.0m Faulkes FLOYDS 2 PTF/CalTech 5.0m Palomar DBSP 1 ------------------------------------------------------------------ PESSTO = Public ESO Spectroscopic Survey for Transient Objects. CSP II = the second Carnegie Supernova Survey. SNfactory = Supernova Factory. LCOGT = Las CumbrasOptical Global Telescopes. PTF = Palomar Transient Factory. NTT = New Technology Telescope. UHT = University of Hawaii Telescope. EFOSC-II = ESO Faint Object Spectrograph and Camera. WFCCD = wide Field CCD Camera. SNIFS = Supernova Integral Field Spectrometer. FLOYDS = Faulkes Low Resolution Spectrograph. DBSP = Double Spectrograph on the 200 Telescope. ------------------------------------------------------------------ The 1m Swope telescope at the Las Campanas Observatory was used to follow the SNe Ia with optical imaging to obtain their light curves. Exposure times were typically 5-10 minutes near peak, longer for fainter supernovae and for supernovae long past peak, with nominally each of six filters, the B,V (Bessell 1990PASP..102.1181B), and the SDSS u, g, r and i. The 2.5m du Pont telescope, also located at the Las Campanas Observatory in Chile, has been used both to take spectra to classify supernova candidates and to take the final template images of the host galaxy after the supernova has faded to allow the subtraction of the host galaxy light from the measured light curve. (2 data files).- Publication:
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VizieR Online Data Catalog
- Pub Date:
- August 2015
- DOI:
- 10.26093/cds/vizier.22190013
- Bibcode:
- 2015yCat..22190013W
- Keywords:
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- Photometry: UBV;
- Photometry: SDSS;
- Supernovae;
- Redshifts;
- Surveys